DOCSLIB.ORG

The Galactic O-Star Spectroscopic Survey (GOSSS). III. 142 Additional

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
The Galactic O-Star Spectroscopic Survey (GOSSS). III. 142 Additional The Galactic O-Star Spectroscopic Survey (GOSSS). III. 142 additional O-type systems1 J. Ma´ızApell´aniz2,3,4,5 Centro de Astrobiolog´ıa, CSIC-INTA, campus ESAC, camino bajo del castillo s/n, E-28 692 Madrid, Spain A. Sota2,3,4 Instituto de Astrof´ısica de Andaluc´ıa-CSIC, Glorieta de la Astronom´ıa s/n, E-18 008 Granada, Spain J. I. Arias, R. H. Barb´a2 Departamento de F´ısica, Universidad de La Serena, Av. Cisternas 1200 Norte, La Serena, Chile N. R. Walborn Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21 218, USA S. Sim´on-D´ıaz Instituto de Astrof´ısica de Canarias, E-38 200 La Laguna, Tenerife, Spain Departamento de Astrof´ısica, Universidad de La Laguna, E-38 205 La Laguna, Tenerife, Spain I. Negueruela DFISTS, EPS, Universidad de Alicante, carretera San Vicente del Raspeig s/n, E-03 690 Alicante, Spain A. Marco DFISTS, EPS, Universidad de Alicante, carretera San Vicente del Raspeig s/n, E-03 690 Alicante, Spain Dept. of Astronomy, University of Florida, 211 Bryant Space Science Center, Gainesville, FL 32 611, USA J. R. S. Le˜ao Univ. Federal do Rio Grande do Norte - UFRN, Caixa Postal 1524, CEP 59 078-970, Natal - RN, Brazil A. Herrero Instituto de Astrof´ısica de Canarias, E-38 200 La Laguna, Tenerife, Spain Departamento de Astrof´ısica, Universidad de La Laguna, E-38 205 La Laguna, Tenerife, Spain R. C. Gamen Instituto de Astrof´ısica de La Plata (CONICET, UNLP), Paseo del Bosque s/n, 1900 La Plata, Argentina E. J. Alfaro Instituto de Astrof´ısica de Andaluc´ıa-CSIC, Glorieta de la Astronom´ıa s/n, E-18 008 Granada, Spain ABSTRACT This is the third installment of GOSSS, a massive spectroscopic survey of Galactic O stars, based on new homogeneous, high signal-to-noise ratio, R ∼ 2500 digital observations selected from the Galactic O-Star Catalog (GOSC). In this paper we present 142 additional stellar systems with O stars from both hemispheres, bringing the total of O-type systems published within the project to 590. Among the new objects there are 20 new O stars. We also identify 11 new double-lined arXiv:1602.01336v2 [astro-ph.SR] 8 Feb 2016 spectroscopic binaries (SB2s), of which 6 are of O+O type and 5 of O+B type, and an additional new tripled-lined spectroscopic binary (SB3) of O+O+B type. We also revise some of the previous GOSSS classifications, present some egregious examples of stars erroneously classified as O-type in the past, introduce the use of luminosity class IV at spectral types O4-O5.5, and adapt the classification scheme to the work of Arias et al. (2016). Subject headings: binaries:spectroscopic — binaries:visual — stars:early type — stars:emission line,Be — surveys 1The GOSSS spectroscopic data in this article were William Herschel Telescope (WHT) and 10.4 m Gran Tele- gathered with five facilities: the 1.5 m Telescope at the Ob- scopio Canarias (GTC) at Observatorio del Roque de los servatorio de Sierra Nevada (OSN), the 2.5 m du Pont Tele- Muchachos (ORM). scope at Las Campanas Observatory (LCO), the 3.5 m Tele- 2Visiting Astronomer, LCO, Chile. scope at Calar Alto Observatory (CAHA), and the 4.2 m 3Visiting Astronomer, CAHA, Spain. 1 1. Introduction graph at the Las Campanas (LCO) 2.5 m du Pont telescope). Starting with paper II, some spec- The Galactic O-Star Spectroscopic Survey tra were also obtained with the ISIS spectrograph (GOSSS) is a long-term project that is obtain- at the 4.2 m William Herschel Telescope (WHT) ing homogeneous, high SNR, R ∼ 2500, blue- at the Observatorio del Roque de los Muchachos violet spectra of a large number (1000+) of (ORM) in La Palma, Spain. In this paper we use O stars in the Milky Way and deriving accu- data from all of the above instruments and we also rate and self-consistent spectral types for all of add a new one, OSIRIS, at the 10.4 m Gran Tele- them (Ma´ızApell´aniz et al. 2011). In Sota et al. scopio Canarias (GTC) at the ORM (Table 1). (2011), from now on paper I, we presented the Only a few GTC spectra are used here but the first installment of the survey, which was com- ◦ number will increase in future GOSSS papers, as prised of the results for 178 northern (δ > −20 ) we have already acquired data for over 200 stars, O stars. In Sota et al. (2014), from now on paper most of them too dim to be accessible with the II, we extended the sample to the southern hemi- other telescopes mentioned above. One difference sphere for a total of 448 O stars. Papers I and between the GTC setup and the rest is that we use II concentrated on the brightest O stars with the two volume-phased holographic gratings, R2500U aim of achieving completeness down to B = 8 but and R2500V, allowing us to cover a larger wave- they also included many dimmer stars. This third length range than with the other instruments. The paper continues the previous work by adding 142 exposures for the two gratings are taken consecu- new stars and raising the sample size to 590. Most tively, with the time difference between the first of the new stars are of luminosity class V, which one and the last one being always less than one are relevant to the OVz phenomenon (Arias et al. hour in order to avoid changes in the phase of 2016), but objects of other luminosity classes are rapidly moving spectroscopic binaries. As we do also included. with the rest of the spectrographs, we use checks This paper is organized as follows. We first to compare that the quality of the data from all present the changes in the observational setup and the spectrographs is uniform and, in those cases the classification scheme in section 2. Then, the where the spectral resolution is higher than 2500, spectral classifications are shown in section 3, di- we degrade it to that value. vided in updates to O stars present in papers I We have also started taking GOSSS data with and II, new O stars, and late-type stars previously [a] the GMOS spectrograph at the 8.1 m Gemini misclassified as of O type. Finally, in section 4 we South telescope, [b] the Goodman High Through- analyze the status of the project based on the new put Spectrograph at the 4.1 m SOAR Telescope spectral classifications. (both at Cerro Pach´on, Chile), and [c] FRO- DOspec at the 2.0 m Liverpool Telescope (at the 2. Data and methods ORM) but we do not use them in this paper; their first GOSSS spectra will likely appear in a future 2.1. Blue-violet spectroscopy with R ∼ 2500 paper IV. The GOSSS data were described in papers I and The GOSSS data in this paper were obtained II and the reader is referred there for further in- between 2007 and 2015. The OSN and LCO ob- formation. Here we detail the changes from those servations were obtained in visitor mode, the GTC previous works. observations in service mode, and the CAHA ob- Most of the spectra presented in paper I were servations in a combination of both. For some SB2 obtained with the Albireo (Observatorio de Sierra and SB3 spectroscopic binaries, multiple epochs Nevada - OSN - 1.5 m telescope) and TWIN (Calar were obtained to observe the different orbit phases. Alto - CAHA - 3.5 m telescope) spectrographs. On In cases with known orbits, observations near the other hand, most of the spectra in paper II quadrature were attempted. were obtained with the Boller & Chivens spectro- The spectral classifications which are the main content of this paper are presented in Ta- 4 Visiting Astronomer, WHT, Spain. bles 4, 5, and 6 and they were obtained with MGB 5 e-mail contact: [email protected]. Ma´ızApell´aniz et al. (2012, 2015c). 2 Table 1: Telescopes, instruments, and settings used in this paper. Telescope Spectrograph Grating Spectral scale Spatial scale Wav. range (A/px)˚ (′′/px) (A)˚ LCO 2.5 m (du Pont) Boller & Chivens 1200 0.80 0.71 3900−5500 OSN 1.5 m Albireo 1800 0.62 0.83 3750−5070 CAHA 3.5 m TWIN (blue arm) 1200 0.55 0.58 3930−5020 ORM 4.2 m (WHT) ISIS (blue arm) 600 0.44 0.20 3900−5600 ORM10.4m(GTC) OSIRIS 2500U 0.62 0.25 3440−4610 2500V 0.80 0.25 4500−6000 2.2. Cataloguing 2.3. Spectral classification methodology and the new standard grid The spectral types are available through the lat- est version (currently v3.2) of the Galactic O-Star The spectral classification methodology was Catalog (GOSC, Ma´ızApell´aniz et al. 2004), ac- laid out in paper I and some changes were pre- cessible at http://gosc.iaa.es. Starting in ver- sented in paper II. Here we introduce two addi- sion 3, the GOSSS spectral types are the default tional changes. ones and the basis for the catalog selection, though The first one concerns the OVz phenomenon, older classifications and those obtained with high- described in detail in Sab´ın-Sanjuli´an et al. (2014) resolution spectra are also kept as possible addi- and Arias et al. (2016). OVz stars have deep tional columns. B- and J-band photometry are He ii λ4686 absorption lines, likely caused primar- 1 also provided in GOSC for all stars . The rec- ily by their extreme youth, though additional fac- tified GOSSS spectra can also be obtained from tors may also play a role.
Load more

Recommended publications
  • Filter Performance Comparisons for Some Common Nebulae
    Filter Performance Comparisons For Some Common Nebulae By Dave Knisely Light Pollution and various “nebula” filters have been around since the late 1970’s, and amateurs have been using them ever since to bring out detail (and even some objects) which were difficult to impossible to see before in modest apertures. When I started using them in the early 1980’s, specific information about which filter might work on a given object (or even whether certain filters were useful at all) was often hard to come by. Even those accounts that were available often had incomplete or inaccurate information. Getting some observational experience with the Lumicon line of filters helped, but there were still some unanswered questions. I wondered how the various filters would rank on- average against each other for a large number of objects, and whether there was a “best overall” filter. In particular, I also wondered if the much-maligned H-Beta filter was useful on more objects than the two or three targets most often mentioned in publications. In the summer of 1999, I decided to begin some more comprehensive observations to try and answer these questions and determine how to best use these filters overall. I formulated a basic survey covering a moderate number of emission and planetary nebulae to obtain some statistics on filter performance to try to address the following questions: 1. How do the various filter types compare as to what (on average) they show on a given nebula? 2. Is there one overall “best” nebula filter which will work on the largest number of objects? 3.
    [Show full text]
  • 2015-AAAP-Photo-Contest
    2015 Kevin J. Brunelle Astrophotography Contest 15 photographers 91 images Atmospheric 10 photographers 20 images Matt Dieterich - Lenticular Clouds over Mt. Rainier Laura Quinn - Lightning Matt Dieterich - Rainier Sunset Laura Quinn - Pittsburgh Clouds Mike Christeson - Angelic Cloud Diane Yorkshire - Mountain Rainbow - Denali Mike Christeson - double rainbow Eric Fischer - Feathery Sundog Frank Wielgus - Scenic Sun and Sundog Eric Fischer - Solitary Ray Over Mingo Diane Yorkshire - Sitka Sunset Diane Yorkshire - Sunset - Inside Passage Len Marraccini - Atlantic Dawn Mike Christeson - Furnace sun set Rich McLaughlin - Morning Sunrise Sky Len Marraccini - Dawn's early rays Mike Christeson - Flowing river Sun Set Diane Yorkshire - Moon over Glacier Bay Julie Yorkshire - The Eclipse Begins from 35000 feet Mark Arelt - Summer Meteor Stellar 9 photographers 19 images Matt Dieterich - Aurora and Milky Way over Mt. Rainier Alexis Kwasinski - Pleiades and comet C2014 Q2 Lovejoy Matt Dieterich - Perseid Meteors and Milky Way over Mt. Rainier Chris Boretzky - Orion Constellation with M42 Mike Christeson- Good Morning Orion Mark McConaughy - Albireo Double Star Mark Arelt - Nocturnal Whirl Alexis Kwasinski - Milky Way Meteor two satellites and green and purple airglow Frank Wielgus - Cygnus Star Cloud Len Marraccini - Milky Way over Bodie Island Nathan Brandt - Milky Way Star Party Frank Wielgus - Brocchi's Cluster Nathan Brandt - Cluster NGC 7686 Mark McConaughy - M13 Globular Cluster Frank Wielgus - Gamma Cassiopeiae and Stellar Friends Nathan
    [Show full text]
  • Rotating Elephant Trunks
    A&A 454, 201–212 (2006) Astronomy DOI: 10.1051/0004-6361:20054494 & c ESO 2006 Astrophysics Rotating elephant trunks G. F. Gahm1,P.Carlqvist2,L.E.B.Johansson3,andS.Nikolic´4,5 1 Stockholm Observatory, AlbaNova University Centre, 106 91 Stockholm, Sweden e-mail: [email protected] 2 Alfvén Laboratory, Royal Institute of Technology, 100 44 Stockholm, Sweden 3 Onsala Space Observatory, 439 92 Onsala, Sweden 4 Departamento de Astronomía, Universidad de Chile, Casilla 36D, Santiago, Chile 5 Astronomical Observatory, Volgina 7, 11060 Belgrade, Serbia and Montenegro Received 8 November 2005 / Accepted 26 January 2006 ABSTRACT Aims. We investigate the structure and velocity of cold molecular pillars, “elephant trunks”, in expanding H ii regions. Methods. The trunks are seen in silhouette against the bright background in our Hα images. All trunks are filamentary, and show signs of being twisted. Four such trunks in NGC 7822, IC 1805, the Rosette Nebula, and DWB 44 were selected, and then mapped mainly in 12CO and 13CO. We determine the mass and density of the trunks. Most of the mass is concentrated in a head facing the central cluster, and in sub-filaments forming the body of the trunk that is connected to V-shaped filaments to the outer expanding shell. Results. We discovered that all four trunks rotate as rigid bodies (to a first approximation) about their major axes, and that at least two trunks are stretching along their major axes, meaning that the massive heads are lagging behind in the general expansion of the H ii regions. The rotational periods are of the order of a few million years – similar to the age of the clusters.
    [Show full text]
  • N O T I C E This Document Has Been Reproduced From
    N O T I C E THIS DOCUMENT HAS BEEN REPRODUCED FROM MICROFICHE. ALTHOUGH IT IS RECOGNIZED THAT CERTAIN PORTIONS ARE ILLEGIBLE, IT IS BEING RELEASED IN THE INTEREST OF MAKING AVAILABLE AS MUCH INFORMATION AS POSSIBLE P993-198422 International Collogium on Atomic Spectra and Oscillator Strengths for Astrophysical and Laboratory Plasmas (4th) Held at the National institute of Standards and Technology Gaithersburg, Maryland on September 14-17, 1992 (U.S.) National inst. of Standards and Technology (PL) Gaithersburg, MD Apr 93 US. DEPARTMENT OF COMMERCE Ndioul Techcical IMermeNON Service B•11G 2-10i1A2 2 MIST-1 /4 U.S. VZPARTMENT OF COMMERCE (REV. NATIONAL INSTITUTE OF STANDARDS AND TECHNOLOGY M GONTSOLw1N^BENN O4" COMM 4M /. MANUSCRIPT REVIEW AND APPROVAL "KIST/ p-850 ^' THIS NSTRUCTWNS: ATTACH ORIGINAL OF FORM TO ONE (1) COPY OF MANUSCIIN IT AND SEINE TO: PUBLICATIOM OATS NUMBER PRINTED PAGES April 1993 199 HE SECRETAIIY, APPROPRIATE EDITO RIAL REVIEW BOARD. ITLE AND SUBTITLE (CITE NN PULL) 4rh International Colloquium on Atomic Spectra and Oscillator Strengths for Astrophysical and Laboratory Plasmas -- POSTER PAPERS :ONTIEACT OR GRANT NUMBER TYPE OF REPORT AND/OR PERIOD COMM UTHOR(S) (LAST %,TAME, POST NNITIAL, SECOND INITIAL) PERFORM" ORGANIZATION (CHECK (IQ ONE SOX) EDITORS XXX MIST/GAITHERSBUIIG Sugar, Jack and Leckrone, B:;vid INST/BODUM JILA BOIRDE11 "ORATORY AND DIVISION NAMES (FIRST MOST AUTHOR ONLY) Physics Laboratory/Atomic Physics Division 'PONSORING ORGANIZATION NAME AND COMPLETE ADDRESS TREET, CITY. STATE. ZNh ^y((S/ ,T AiL7A - -ASO IECOMMENDsO FOR MIST PUBLICATION JOVIAMAL OF RESEMICM (MIST JRES) CIONOGRAPK (MIST MN) LETTER CIRCULAR J. PHYS. A CHEM.
    [Show full text]
  • WISE Captures a Cosmic Rose 16 March 2010
    WISE Captures a Cosmic Rose 16 March 2010 supernova remnant associated with this region, called NGC 7822, indicates that a massive star has already exploded, blowing the cloud open in a "champagne flow" and leaving behind this floral remnant. Blue dots sprinkled throughout are foreground stars in our Milky Way galaxy. Berkeley 59 and NGC 7822 are located in the constellation of Cepheus at a distance of about 3,300 light-years from Earth. Infrared light is color coded in this picture as follows: blue shows 3.4-micron light; cyan, 4.6-micron light; green, 12-micron light; and red, 22-micron light. A new infrared image from NASA's Wide-field Infrared Provided by JPL/NASA Survey Explorer, or WISE, shows a cosmic rosebud blossoming with new stars. Image credit: NASA/JPL- Caltech/UCLA (PhysOrg.com) -- A new infrared image from NASA's Wide-field Infrared Survey Explorer, or WISE, shows a cosmic rosebud blossoming with new stars. The stars, called the Berkeley 59 cluster, are the blue dots to the right of the image center. They are ripening out of the dust cloud from which they formed, and at just a few million years old, are young on stellar time scales. The rosebud-like red glow surrounding the hot, young stars is warm dust heated by the stars. Green "leafy" nebulosity enfolds the cluster, showing the edges of the dense, dusty cloud. This green material is from heated polycyclic aromatic hydrocarbons, molecules that can be found on Earth in barbecue pits, exhaust pipes and other places where combustion has occurred.
    [Show full text]
  • Astronomy Magazine Special Issue
    γ ι ζ γ δ α κ β κ ε γ β ρ ε ζ υ α φ ψ ω χ α π χ φ γ ω ο ι δ κ α ξ υ λ τ μ β α σ θ ε β σ δ γ ψ λ ω σ η ν θ Aι must-have for all stargazers η δ μ NEW EDITION! ζ λ β ε η κ NGC 6664 NGC 6539 ε τ μ NGC 6712 α υ δ ζ M26 ν NGC 6649 ψ Struve 2325 ζ ξ ATLAS χ α NGC 6604 ξ ο ν ν SCUTUM M16 of the γ SERP β NGC 6605 γ V450 ξ η υ η NGC 6645 M17 φ θ M18 ζ ρ ρ1 π Barnard 92 ο χ σ M25 M24 STARS M23 ν β κ All-in-one introduction ALL NEW MAPS WITH: to the night sky 42,000 more stars (87,000 plotted down to magnitude 8.5) AND 150+ more deep-sky objects (more than 1,200 total) The Eagle Nebula (M16) combines a dark nebula and a star cluster. In 100+ this intense region of star formation, “pillars” form at the boundaries spectacular between hot and cold gas. You’ll find this object on Map 14, a celestial portion of which lies above. photos PLUS: How to observe star clusters, nebulae, and galaxies AS2-CV0610.indd 1 6/10/10 4:17 PM NEW EDITION! AtlAs Tour the night sky of the The staff of Astronomy magazine decided to This atlas presents produce its first star atlas in 2006.
    [Show full text]
  • DSLR PHOTOMETRY: a Citizen Science Project Using a Consumer Camera to Contribute Scientific Data
    DSLR PHOTOMETRY: A citizen science project using a consumer camera to contribute scientific data by Mike Durkin Photometry is one of many areas in astronomy where amateurs can make useful contributions. Other areas include astrometry, occultation timings, and recording high quality observations of solar system objects. There are also projects for “armchair astronomers”, such as Galaxy Zoo. What is Photometry? Photometry is the measurement and study of the brightness of objects In astronomy, photometry is used to measure the brightness of stars , supernovae, asteroids , etc. I will be talking mostly about measuring variable stars , which are stars that change brightness over time. By studying the how the brightness of objects change over time, it can help determine physical properties. LIGHT CURVE shows brightness changes over time Cepheids are a type of variable stars that fluctuate in brightness. There is a well defined relationship between brightness and the Period of the brightness variation. Cepheids were used to determine the distance to the Andromeda Galaxy and proved that the universe was much larger than just the Milky Way. Light Curve for an asteroid can be used to show rotational period. Light curve for eclipsing binary The light curve for an eclipsing binary can be used to determine properties such as the diameters, luminosities, and separation of the stars. Eclipsing binary star animation courtesy of Wikimedia Commons THIS SOUNDS LIKE STUFF FOR PROFESSIONAL ASTRONOMERS, WHAT GOOD CAN AMATEURS DO? There are a lot more amateurs than professionals Estimated total number of professional astronomers is 2,080 (U.S. Dept. of Labor, Bureau of Labor Statistics) Estimated total number of amateurs is at least 100,000 based on the circulation numbers of magazines.
    [Show full text]
  • Übersicht NGC-Objektauswahl Cepheus Zur Übersichtskarte
    NGC-Objektauswahl Cepheus NGC 40 NGC 7055 NGC 7354 NGC 188 NGC 7076 NGC 7380 NGC 1184 NGC 7129 NGC 7419 NGC 1544 NGC 7139 NGC 7423 NGC 2276 NGC 7142 NGC 7429 NGC 2300 NGC 7160 NGC 7510 NGC 6939 NGC 7226 NGC 7538 NGC 6949 NGC 7235 NGC 7708 NGC 6951 NGC 7261 NGC 7762 NGC 7023 NGC 7281 NGC 7822 Sternbild- Übersicht Zur Objektauswahl: Nummer anklicken Zur Übersichtskarte: Objekt anklicken Sternbildübersicht Auswahl NGC 40_7708 Aufsuchkarte Auswahl NGC 188_Aufsuchkarte 2 UMi 2 Auswahl NGC 1184 Aufsuchkarte Auswahl NGC 1544_2276_2300 Aufsuchkarte Auswahl NGC 6939 Aufsuchkarte Auswahl NGC 6949_6951 Aufsuchkarte Auswahl NGC 7023 Aufsuchkarte Auswahl NGC 7055 Aufsuchkarte Auswahl NGC 7076 Aufsuchkarte Auswahl NGC 7129_7142 Aufsuchkarte Auswahl NGC 7139_7160 Aufsuchkarte Auswahl NGC 7226_7235 Aufsuchkarte Auswahl N 7261_7281 Aufsuchkarte Auswahl NGC 7354_7419_7429_7510_7538 Aufsuchkarte Auswahl NGC 7380_7423 Aufsuchkarte Auswahl NGC 7762_7822 Aufsuchkarte Auswahl NGC 40 Übersichtskarte Aufsuch- Auswahl karte NGC 188 Übersichtskarte Aufsuch- Auswahl karte NGC 1184 Übersichtskarte Aufsuch- Auswahl karte NGC 1544 Übersichtskarte Aufsuch- Auswahl karte N 2276_N 2300 Übersichtskarte Aufsuch- Auswahl karte NGC 6939 Übersichtskarte Aufsuch- Auswahl karte NGC 6949 Übersichtskarte Aufsuch- Auswahl karte NGC 6951 Übersichtskarte Aufsuch- Auswahl karte NGC 7023 Übersichtskarte Aufsuch- Auswahl karte NGC 7055 Übersichtskarte Aufsuch- Auswahl karte NGC 7076 Übersichtskarte Aufsuch- Auswahl karte NGC 7129_7142 Übersichtskarte Aufsuch- Auswahl karte NGC 7139
    [Show full text]
  • Orbital Elements of Double Stars
    Orbital elements of double stars: ADS 1548 Marco Scardia, Jean-Louis Prieur, Luigi Pansecchi, Robert Argyle, Josefina Ling, Eric Aristidi, Alessio Zanutta, Lyu Abe, Philippe Bendjoya, Jean-Pierre Rivet, et al. To cite this version: Marco Scardia, Jean-Louis Prieur, Luigi Pansecchi, Robert Argyle, Josefina Ling, et al.. Orbital elements of double stars: ADS 1548. 2018, pp.1. hal-02357208 HAL Id: hal-02357208 https://hal.archives-ouvertes.fr/hal-02357208 Submitted on 23 Nov 2019 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. INTERNATIONAL ASTRONOMICAL UNION COMMISSION G1 (BINARY AND MULTIPLE STAR SYSTEMS) DOUBLE STARS INFORMATION CIRCULAR No. 194 (FEBRUARY 2018) NEW ORBITS ADS Name P T e Ω(2000) 2018 Author(s) α2000δ n a i ! Last ob. 2019 1548 A 819 AB 135y4 2011.06 0.548 153◦8 39◦7 000161 SCARDIA 01570+3101 2◦6587 000424 50◦5 189◦7 2017.833 49.4 0.163 et al. (*) - HDS 333 49.54 1981.14 0.60 252.6 253.8 0.542 TOKOVININ 02332-5156 7.2665 0.413 57.4 150.9 2018.073 255.7 0.519 - COU 691 61.76 1964.53 0.059 68.6 276.2 0.109 DOCOBO 03423+3141 5.8290 0.160
    [Show full text]
  • THE NICKEL MASS DISTRIBUTION of NORMAL TYPE II SUPERNOVAE 3 Supernova Are the Magnitudes in Different filters, the Pho- Above
    DRAFT VERSION MAY 17, 2017 Preprint typeset using LATEX style emulateapj v. 12/16/11 THE NICKEL MASS DISTRIBUTION OF NORMAL TYPE II SUPERNOVAE ∗ TOMAS´ MULLER¨ 1,2 , JOSE´ L. PRIETO1,3,ONDREJˇ PEJCHA4 AND ALEJANDRO CLOCCHIATTI1,2 1 Millennium Institute of Astrophysics, Santiago, Chile 2 Instituto de Astrof´ısica, Pontificia Universidad Cat´olica de Chile, Av. Vicua Mackenna 4860, 782-0436 Macul, Santiago, Chile 3 N´ucleo de Astronom´ıa de la Facultad de Ingenier´ıa y Ciencias, Universidad Diego Portales, Av. Ej´ercito 441, Santiago, Chile 4 Lyman Spitzer Jr. Fellow, Department of Astrophysical Sciences, Princeton University, 4 Ivy Lane, Princeton, NJ 08540, USA Draft version May 17, 2017 ABSTRACT Core-collapse supernova explosions expose the structure and environment of massive stars at the moment of their death. We use the global fitting technique of Pejcha & Prieto (2015a,b) to estimate a set of physical pa- 56 rameters of 19 normal Type II SNe, such as their distance moduli, reddenings, Ni masses MNi, and explosion energies Eexp from multicolor light curves and photospheric velocity curves. We confirm and characterize known correlations between MNi and bolometric luminosity at 50 days after the explosion, and between MNi and Eexp. We pay special attention to the observed distribution of MNi comingfrom a jointsampleof 38 TypeII SNe, which can be described as a skewed-Gaussian-like distribution between 0.005 M⊙ and 0.280 M⊙, with a median of 0.031 M⊙, mean of 0.046 M⊙, standard deviation of 0.048 M⊙ and skewness of 3.050. We use two- sample Kolmogorov-Smirnov test and two-sample Anderson-Darling test to compare the observed distribution of MNi to results from theoretical hydrodynamical codes of core-collapse explosions with the neutrino mech- anism presented in the literature.
    [Show full text]
  • Three Editions of the Star Catalogue of Tycho Brahe*
    A&A 516, A28 (2010) Astronomy DOI: 10.1051/0004-6361/201014002 & c ESO 2010 Astrophysics Three editions of the star catalogue of Tycho Brahe Machine-readable versions and comparison with the modern Hipparcos Catalogue F. Verbunt1 andR.H.vanGent2,3 1 Astronomical Institute, Utrecht University, PO Box 80 000, 3508 TA Utrecht, The Netherlands e-mail: [email protected] 2 URU-Explokart, Faculty of Geosciences, Utrecht University, PO Box 80 115, 3508 TC Utrecht, The Netherlands 3 Institute for the History and Foundations of Science, PO Box 80 000, 3508 TA Utrecht, The Netherlands Received 6 January 2010 / Accepted 3 February 2010 ABSTRACT Tycho Brahe completed his catalogue with the positions and magnitudes of 1004 fixed stars in 1598. This catalogue circulated in manuscript form. Brahe edited a shorter version with 777 stars, printed in 1602, and Kepler edited the full catalogue of 1004 stars, printed in 1627. We provide machine-readable versions of the three versions of the catalogue, describe the differences between them and briefly discuss their accuracy on the basis of comparison with modern data from the Hipparcos Catalogue. We also compare our results with earlier analyses by Dreyer (1916, Tychonis Brahe Dani Scripta Astronomica, Vol. II) and Rawlins (1993, DIO, 3, 1), finding good overall agreement. The magnitudes given by Brahe correlate well with modern values, his longitudes and latitudes have error distributions with widths of 2, with excess numbers of stars with larger errors (as compared to Gaussian distributions), in particular for the faintest stars. Errors in positions larger than 10, which comprise about 15% of the entries, are likely due to computing or copying errors.
    [Show full text]
  • Time, Spatial, and Spectral Resolution of the Halpha Line-Formation Region of Deneb and Rigel with the VEGA/CHARA Interferometer
    Astronomy & Astrophysics manuscript no. AB˙Supergiants˙vResubmission˙vEnglishCorr˙Printer c ESO 2018 October 11, 2018 Time, spatial, and spectral resolution of the Hα line-formation region of Deneb and Rigel with the VEGA/CHARA interferometer ⋆ O. Chesneau1, L. Dessart2 D. Mourard1, Ph. B´erio1, Ch. Buil3, D. Bonneau1, M. Borges Fernandes1,9, J.M. Clausse1, O. Delaa1, A. Marcotto1, A. Meilland4, F. Millour4, N. Nardetto1, K. Perraut5, A. Roussel1, A. Spang1, P. Stee1, I. Tallon-Bosc6, H. McAlister7,8, T. ten Brummelaar8, J. Sturmann8, L. Sturmann8, N. Turner8, C. Farrington8 and P.J. Goldfinger8 1 UMR 6525 H. Fizeau, Univ. Nice Sophia Antipolis, CNRS, Observatoire de la Cˆote d’Azur, Av. Copernic, F-06130 Grasse, France 2 Laboratoire d’Astrophysique de Marseille, Universit´ede Provence, CNRS, 38 rue Fr´ed´eric Joliot-Curie, F-13388 Marseille Cedex 13, France 3 Castanet Tolosan Observatory, 6 place Clemence Isaure, 31320 Castanet Tolosan, France 4 Max-Planck Institut f¨ur Radioastronomie, Auf dem Hugel 69, 53121, Bonn, Germany 5 Laboratoire d’Astrophysique de Grenoble (LAOG), Universit´eJoseph-Fourier, UMR 5571 CNRS, BP 53, 38041 Grenoble Cedex 09, France 6 Univ. Lyon 1, Observatoire de Lyon, 9 avenue Charles Andr´e, Saint-Genis Laval, F-69230, France 7 Georgia State University, P.O. Box 3969, Atlanta GA 30302-3969, USA 8 CHARA Array, Mount Wilson Observatory, 91023 Mount Wilson CA, USA 9 Observat´orio Nacional, Rua General Jos´eCristino, 77, 20921-400, S˜ao Cristov˜ao, Rio de Janeiro, Brazil Received, accepted. ABSTRACT Context. BA-type supergiants are amongst the most optically-bright stars.
    [Show full text]